Notes. ^(a) Positions of the 1.3 mm continuum peak emission are extracted from the CALYPSO dataset (Maury et al. 2019). ^(b) Systemic velocities, V_sys, correspond to the mean velocity of C¹⁸O (2− 1) emission on the source continuum peak position as fit by Maret et al. (2020), except for GF9-2 (from ¹³ CO (2− 1)), IRAM04191 (Belloche et al. 2002), L1521-F (from NH₃ (1,1), Codella et al. 1997), and SerpM-SMM4 (from CO (3−2), Dionatos et al. 2010). For multiple systems the systemic velocity of the primary is reported. ^(c) Distances: Ortiz-León et al. (2018a) for the Perseus sources; Zucker et al. (2019) for the Taurus sources and L1157; Ortiz-León et al. (2017, 2018b) for SerpM; Palmeirim et al. (in prep.) for SerpS; C. Zucker (priv. comm.) for GF9-2. For multiple systems the distance of the primary is reported. ^(d)Internal luminosities are derived by Ladjelate et al. (in prep.), from the 70 μm flux from the Herschel Gould Belt survey observations at 8′′ spatial resolution (André et al. 2010), except for GF9-2 for which we use the value by Wiesemeyer et al. (1997) rescaled to the distance given in the fifth column. The uncertainty is in parentheses when available, and is larger for SVS13B because of the proximity to SVS13A. For SerpM-SMM4b the upper limit is given by the bolometric luminosity (Aso et al. 2019). ^(e) Envelope mass from Maury et al. (2019) and references therein. For the binaries with no mass estimate of their individual envelopes, the value corresponds to the fraction of the total envelope mass in proportion of the peak flux densities at 1.3 mm given by Maury et al. (2019). The masses have been re-scaled to the distances given in Col. 5. ^(f) The classification as Class 0, I, or candidate protostellar object (in parentheses) is based on Maury et al. (2019). ^(*) For SerpM-S68Nb and SerpM-S68Nc we follow the same naming as Maury et al. (2019). The names of the two sources are inverted with respect to the classification by Williams & Myers (2000), also followed by Dionatos et al. (2010). ^(**) Protostellar companionswhich lie outside of the primary beam at 231 GHz (~ 21′′).